Some results from an optical Some results from an optical monitoring of four quasars at monitoring of four quasars at Calar Alto Observatory Calar Alto Observatory (Almería, Spain)(Almería, Spain)

Aurora Ullán (UC)Aurora Ullán (UC)

Jan-Erik Ovaldsen (University of Oslo)Jan-Erik Ovaldsen (University of Oslo)

Luis Goicoechea (UC)Luis Goicoechea (UC)

Rolf Stabell (University of Oslo)Rolf Stabell (University of Oslo)

Collaboration:Collaboration:Department of Modern Department of Modern Physics of the University Physics of the University of Cantabria , Santander, of Cantabria , Santander, SpainSpain

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Institute of Theoretical Institute of Theoretical Astrophysics (University of Astrophysics (University of Oslo), Oslo, NorwayOslo), Oslo, Norway

CONTENTSCONTENTS

Introduction: optical monitoring and observationsIntroduction: optical monitoring and observations

The Double Quasar: QSO 0957+561 A,BThe Double Quasar: QSO 0957+561 A,B

SBS 0909+532: another double quasarSBS 0909+532: another double quasar

The two isolated quasars:The two isolated quasars:

- PG1427- PG1427

- PG1626- PG1626

Final conclusionsFinal conclusions

INTRODUCTIONINTRODUCTION We carried out an intensive monitoring in Calar Alto Observatory (Almería, Spain) between 2003 March 3 and 2003 June 2

The scientific interest of our monitoring was to find and study the variability in four targets: two double quasars and two isolated ones

Another interest for us was to test the capability of the EOCA telescope, in order to carry out future programs for gravitational lenses

Telescope: EOCA (1.52m), Telescope: EOCA (1.52m), Calar Alto ObservatoryCalar Alto Observatory

Observer: Aurora UllánObserver: Aurora Ullán

Data analysis: UC & Univ. Data analysis: UC & Univ. OsloOslo

We tried to take at least three different frames for each We tried to take at least three different frames for each system and each night in order to obtain a “local” estimation system and each night in order to obtain a “local” estimation of the errorsof the errors

A typical exposure is 300s in V and 150 in R (in general A typical exposure is 300s in V and 150 in R (in general for all the targets)=> not very long in order to NOT saturate for all the targets)=> not very long in order to NOT saturate the reference starsthe reference stars

We used always R and V Johnson filtersWe used always R and V Johnson filters

The Double Quasar: QSO 0957+561 A,BThe Double Quasar: QSO 0957+561 A,B

QSO 0957+561 A,B

QSO 0957+561 was the first lensed quasar

It was discovered in 1979 by Walsh et al.

It is formed by two images (A and B) from an inner region of a far quasar ( z = 1.41 )

The distance between A and B is 6.1”

The main lens galaxy ( z = 0.36 ) is a giant elliptical one residing in a cluster of galaxies and was discovered by Stockton in 1980

• TWO PHOTOMETRIC METHODS:

- Jan-Erik -> PSF with an IDL task

- Aurora -> psfphot (PSF fitting)

* RESULTS : ALMOST THE SAME!!!

(1) REAL FRAME

(2) MODEL

(1) – (2) = (3)

(3) RESIDUAL

RED-> A COMPONENT BLUE-> B COMPONENT

RED-> A COMPONENT BLUE-> B COMPONENT

EOCA (psfphot) =

EOCA (OSLO) = We compute the diference between each magnitude with the median magnitude for each component ( on each photometry)

We see that the results are very similar....it should be ok!!

We find a big gap between 2720 and 2760......bad weather

WHAT CAN WE DO?

We got some “extra” data (five nights in that gap) of Rudy Schild (Mount Hopkins Observatory)

We will see what happens....

It seems to be an event in the A component with an amplitude less than 50 mmag

It seems to be an event of 60 mmag in the A component

Comparison between both filters

SBS 0909+532: another double quasarSBS 0909+532: another double quasar

z = 1.377

B = 17.0

Separation between images: 1.107 +/- 0.006 arcsec

Despite it is not a very studied system,it is probed that SBS 0909+532 is a gravitational lens

The lens redshift is z = 0.83

SEE BEHAVIOUR

TWO VERY BAD NIGHTS: 2707 AND 2758

IN BOTH FILTERS!!

The two isolated quasars: PG1427 and PG1626The two isolated quasars: PG1427 and PG1626

For these systems we wanted to find variability on time scales of a few days (1-10 days), less than our period of sampling

To test the cromaticity or acromaticity of the variability

To compare with quasars afected by gravitational lensing

PG 1427+48

z = 0.220

PG1626+55

z = 0.133

The structure function in the R band, for an arbitrary lag (temporal separation) is

Ds(1) = (1/2N) ij [(mj – mi)2 – i

2 – j2] ,

for pairs (i,j) that verify tj – ti lag (N 2).

SFk is k2 SF (SF is the intrinsic structure function of L, NOT of apparent magnitude)

m (obs) k L (cte luminosity)

t (obs) T (rest frame time)

N 6 K= f()

THE END